2004AJ....127.3537S


C.D.S. - SIMBAD4 rel 1.7 - 2021.04.16CEST11:31:43

2004AJ....127.3537S - Astron. J., 127, 3537-3552 (2004/June-0)

X-ray properties of pre-main-sequence stars in the Orion nebula cluster with known rotation periods.

STASSUN K.G., ARDILA D.R., BARSONY M., BASRI G. and MATHIEU R.D.

Abstract (from CDS):

We reanalyze all archival Chandra/ACIS observations of the Orion Nebula Cluster (ONC) to study the X-ray properties of a large sample of pre-main-sequence (PMS) stars with optically determined rotation periods. Our goal is to elucidate the origins of X-rays in PMS stars by seeking out connections between the X-rays and the mechanisms most likely driving their production–rotation and accretion. Stars in our sample have LX/Lbolnear, but below, the ``saturation'' value of 10–3. In addition, in this sample X-ray luminosity is significantly correlated with stellar rotation, in the sense of decreasing LX/Lbolwith more rapid rotation. These findings suggest that stars with optical rotation periods are in the ``super-saturated'' regime of the rotation-activity relationship, consistent with their Rossby numbers. However, we also find that stars with optical rotation periods are significantly biased to high LX. This is not the result of magnitude bias in the optical rotation-period sample, but rather of the diminishingly small amplitude of optical variations in stars with low LX. Evidently, there exists in the ONC a population of stars whose rotation periods are unknown and that possess lower average X-ray luminosities than those of stars with known rotation periods. These stars may sample the linear regime of the rotation-activity relationship. Accretion also manifests itself in X-rays, though in a somewhat counterintuitive fashion: while stars with spectroscopic signatures of accretion show harder X-ray spectra than nonaccretors, they show lower X-ray luminosities and no enhancement of X-ray variability. We interpret these findings in terms of a common origin for the X-ray emission observed from both accreting and nonaccreting stars, with the X-rays from accreting stars simply being attenuated by magnetospheric accretion columns. This suggests that X-rays from PMS stars have their origins primarily in chromospheres, not accretion.

Abstract Copyright:

Journal keyword(s): Stars: Pre-Main-Sequence - Stars: Rotation - X-rays

Simbad objects: 11

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Number of rows : 11

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 NAME Tau-Aur Complex SFR 04 30 +25.0           ~ 1251 0
2 NAME Orion Nebula Cluster OpC 05 35.0 -05 29           ~ 2050 1
3 * tet01 Ori C ** 05 35 16.4664092288 -05 23 22.897102710 4.20 5.15 5.13 4.91 4.73 O7Vp 1299 1
4 NAME Trapezium Cluster As* 05 35 16.5 -05 23 14           ~ 1505 1
5 OMC 3 MoC 05 35 20.0 -05 01 00           ~ 234 1
6 OMC 2 MoC 05 35 27 -05 10.1           ~ 404 1
7 NGC 2264 OpC 06 40 58 +09 53.7           ~ 1622 0
8 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1611 1
9 NAME TW Hya Association As* 11 01.9 -34 42           ~ 843 0
10 NAME Cha 1 MoC 11 06 48 -77 18.0           ~ 1014 1
11 NAME ASSOC II SCO As* 16 15 -24.2           ~ 1168 1

    Equat.    Gal    SGal    Ecl

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2021.04.16-11:31:43

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